1. Convective throughout deliver heat from core to surface purely by convection.

Size: px
Start display at page:

Download "1. Convective throughout deliver heat from core to surface purely by convection."

Transcription

1 6/30 Post Main Sequence Evolution: Low-Mass Stars 1. Convective throughout deliver heat from core to surface purely by convection. 2. Convection mixes the material of the star is the material carries the heat. 3. Once the H is gone in the center of the star, it is gone everywhere in the star. 4. The star is now all He and can t get hot enough to fuse He into other elements. 5. Once the H is gone, fusion stops. 6. No longer outward radiation pressure; the star begins to gravitationally contract again. 7. Eventually, this contraction stops due to Pauli Repulsion. (Aside: Pauli Exclusion Principle To explain the structure of the periodic table of the elements why different elements have different chemistry hypothesized that electrons could not share the same quantum state. Also true of protons, neutrons, and neutrinos among other particles.) Further contraction of the star would cause electrons to occupy the same quantum states can t happen. Matter in this state is called degenerate electrons occupy all available quantum states. 8. The star is now about the size of the Earth and has become quite hot because of its contraction. 9. It is a white dwarf. 10. The white dwarf sits in space radiating its heat away and eventually becomes a black dwarf. More Massive Stars: Either the star has a radiative core and convective envelope (medium-mass stars such as the Sun) or the star has a convective core and radiative envelope (most massive stars). In either case, there is no mixing between the material in the core and the material in the envelope. Eventually, the hydrogen is used up in the core but, when this happens, there is still H in the envelope.

2 When the H is used up in the core, the core begins to contract. When the core contracts, it gets hotter this causes H fusion into He to start in the envelope. The outflow of energy from this region, because of its low density, causes the envelope to expand. The star expands and cools becomes a red giant. In the lower mass stars among the medium mass star, the core will never get hot enough to fuse He into heavier elements. The outflow of energy in the envelope eventually expels the envelope into space, leaving behind the core of the star. The core of the star contracts until stopped by Pauli repulsion becomes a white dwarf. Our own Sun will get hot enough to fuse He into heavier elements carbon and oxygen. It will spend a short amount of the time on the He main sequence. The Sun will not get hot enough to fuse carbon and oxygen into heavier nuclei. The Sun will also expel its envelope and end up as a white dwarf made of carbon and oxygen. More massive stars will be able to fuse carbon and oxygen into heavier elements. More and more massive stars will eventually form white dwarfs of heavier and heavier elements. Until we get to iron that s the next chapter. We can test these ideas by examining star clusters. Two types of star cluster: 1. Open few stars a few 10's to a few 1000's stars tend to be young where stars are born size about 10 pc irregular shape 2. Globular Star Cluster Many stars 100's of thousands to millions of stars. stars tend to be old may be the oldest structures in the universe sizes 20 to 30 pc name from their spherical shape like a globe

3 Assume that all the stars in a cluster were created at about the same time. We should see different mass stars in clusters at different stages of evolution. Expect to see for an open cluster: 1. No low-mass stars on the main sequence not enough time to evolve that far. 2. Only the most massive stars very few will have evolved off the main sequence. 3. Draw HR diagram for an open cluster. 4. The turn-on point, where stars are just evolving on to the main sequence can be used to deduce the age of the cluster. Expect to see for a globular cluster. 1. Even the lowest mass stars will have had time to evolve onto the main sequence. 2. The massive stars will have had time to evolve off the main sequence. 3. Draw HR diagram for a globular cluster. 4. Turn-off point tells us about the age of the cluster. Chapter 10 The Deaths of Stars We have already discussed the deaths of less massive stars end as white/black dwarfs. Here we discuss the end states of the most massive stars. Chandrasekhar discovered that a white dwarf can be no more massive than 1.4 solar masses if it is, not even Pauli repulsion can prevent further contraction. We will now discuss what happens to stars whose end states have masses greater than the Chandrasekhar limit. The most massive stars, after leaving the main sequence, will continue to fuse elements until they get to iron. Iron is the most stable of nuclei produced inside a star no energy can be generated from fusing iron into heavier elements. When the core of the star becomes iron, fusion stops.

4 In a fraction of a second, the core collapses. The core rebounds like a compressed spring that produces an explosion that tears the star apart supernova. A supernova can be brighter than the galaxy of which it is apart. A type II SN such as this one can be as bright as 600 million Suns. One nearby can be bright enough to shine out in the daytime. A SN within 50 ly of the Earth could destroy all life here on Earth. What is left at the center? Depends on the mass of the star. If the main sequence mass is less than 40 solar masses, the remnant will be between 1.4 solar masses and 2 to 3 solar masses. Since the mass is greater than the Chandrasekhar limit, not even the Pauli repulsion of the electrons can prevent further contraction. The electrons are forced into protons, converting them to neutrons. We end up with a ball of neutrons with a few electrons and protons floating around that continues to contract. But neutrons also must obey the Pauli principle object contracts until further contraction would cause neutrons to occupy the same quantum states. We end up with a neutron star. Characteristics of a Neutron Star Mass about 2 solar masses radius about 10 km like a huge nucleus density is the same as the density of an atomic nucleus because they start big with a slow rotation, the end up small with a rapid rotation about 30 times a second. material of the neutron star behaves like a superconductor magnetic field of the neutron star is trapped in the superconducting matter and rotates around with the star We have found neutron stars first were pulsars that

5 sent rapid pulses of the light in our direction. The magnetic field axis in a neutron star will probably be off the spin axis case here on Earth. Charged particles trapped in the magnetic field send beams of light along the axis of the magnetic field. As the neutron star spins, the beam of light sweeps around. When pointed at Earth, it sends a pulse our way. We see a series of pulses, say, 30 times a second. This is the lighthouse model of a neutron star/pulsar. We can also detect neutron stars in close binary systems neutron star is close enough to its companion to bleed mass off of it. As the matter loses gravitational energy, it converts it to x rays we can detect the x rays. We know it s a neutron star because we know what sort of x ray spectrum we should see from a neutron star. If it is a not close binary system, and we calculate the mass of the unseen companion and if it has the mass of a neutron star, we know it s a neutron star. Gravitational Lens Effect If a neutron star comes between us and distant object, it will cause the distant object to increase in brightness. How much and how long tells us the nature of the impeding object and, with the right properties, it will be a neutron star. Astrometric Binary Star Only see one of the two stars. Analyzing the system will allow us to find the mass of the unseen companion. If that mass is in the range of neutron star masses, it is a neutron star. What if the final mass of the remnant is greater than 2 to 3 solar masses (main sequence mass of more than 40 solar masses)? Not even the Pauli repulsion of the neutrons can prevent further contraction. Gravity takes over and the object contracts without stopping. What goes on until the object gets to be atomic size or so is governed by the general theory of relativity GR. Special Theory of Relativity SR Michaelson-Morely Experiment Hypothesis: electromagnetic waves travel through a medium called the ether.

6 M-M set about finding the motion of the Earth relative to the ether. Compared the speed of a light signal along perpendicular paths. In the figure, suppose that the ether is traveling horizontally toward the right. Light from the source S travels toward mirror M 1, which is a half-silvered mirror. Some of the light passes through toward mirror M 3, where it is reflected back. Some of the light is reflected toward mirror M 2, where it is reflected back. The two beams of light are recombined at mirror M 1, and observed by the observer. If the speed of light is different along the two paths, the observer will see the effect of interference between the two beams. If the ether flows, say, horizontally the right, the horizontal light beam will take less time to complete the trip than the vertical one will. One should see interference and from the amount of interference, the speed of the ether can be deduced. No interference was seen. Found no difference in the speed of light in the two different directions. Two Postulates for the Special Theory of Relativity: 1. The laws of physics are the same in all unaccelerated frames of reference. 2. All observers, regardless of their frame of reference, will measure the same value for the speed of light. Consequences. 1. Simultaneity Two events that are simultaneous in one frame of reference are not necessarily simultaneous in any other frame of reference. Note that, if two events occur simultaneously at the same point in space, they will be simultaneous in all frames. If two events are simultaneous in one frame of reference, they are not necessarily simultaneous in any other frame of reference. Consider the light train in the picture below:

7 Fast train travels through a station without stopping at the platform. We have two observers: T on the train in the middle of the train and P on the platform directly across from T (at the time shown). At the instant shown, two lighting bolts hit the front and rear of the train simultaneously in the frame of P. We have set up the problem so that the bolts strike simultaneously in the platform frame; we will show that they do not strike simultaneously in the train frame. What P sees with regard to the lightning bolts: 1. P sees the light from the bolts arrive at his position at the same time. 2. P sees that the light from the two bolts has traveled the same distance half the length of the train. 3. P measures the speed of the light from both bolts to be the same. 4. P sees the light signals from the two bolts have traveled the same distance in the same time at the same speed, and concludes that the two bolts struck the train at the same time. They are simultaneous in his frame. What P observes about T: 1. P sees T moving toward the light signal from the front bolt and away from the light signal from the rear bolt. 2. P sees the light from the front bolt arrive at T s location before the light from the rear bolt. 3. Since this sequence of events occurs at the same point in T s frame, this sequence of events is the same in both frames.

8 What T sees about the lightning bolts: 1. T sees the light from the front bolt arrive before the light from the rear bolt. 2. T sees that both light signals have traveled the same distance half the length of the train. 3. T measures the speed of the light signals to have the same value (2 nd postulate). 4. T sees the light signals from the two bolts travel the same distance at the same speed. But, since the light from the front bolt arrives first, he concludes that the front bolt occurred first. The bolts aren t simultaneous in T s frame. In Newtonian physics, time is absolute and the same in all frames. But Einstein made the speed of light absolute. Something had to give, and it was absolute time (and, as we will see, space). This suggests that time passes at different rates in the two frames. Time Dilation Consider the light clock. A base containing electronics, a light bulb, and a detector. A pulse is emitted from the light bulb, travels to a mirror, and is reflected back to the detector. The electronics then generates the next pulse. Place an ordinary clock at the location of the light light clock and synchronized with it. Since they are located at the same point in space, they will be synchronized in all frames. We will accelerate ourselves up to a large speed moving to the left. In this frame, the clock will move to the right. Draw the light clock as observed in this new frame.

9 In the new frame, the clock travels from left to right with speed V. In this frame, the light pulse travels a greater distance than it does in the rest frame of the clock. But it does so at the same speed because postulate 2 tells us that speed of light is the same in both frames. It takes longer for the light pulse to get from light bulb to detector in the moving frame. The clock ticks more slowly in the moving frame. Time passes more slowly in the moving frame. Time Dilation: In this formula, the t s are time intervals, one in the rest frame of the clock (the frame in which the clock is at rest) and one in the frame in which the clock is moving. This result has been tested experimentally by accelerating unstable particles called muons to nearly the speed of light. The fast moving muons have longer lifetimes than muons at rest. There is numerical agreement within uncertainty with Einstein s prediction. In fact, this is the reason that muons form about 75% of the secondary

10 cosmic radiation at the surface of the Earth. Their lifetimes are not long enough for them to reach the surface of Earth without time dilation. Showers of muons are created in the upper atmosphere, roughly 100 km up. They travel at nearly the speed of light. They have a lifetime of 2.2 s or 2.2 millionths of a second. Without time dilation, the muons would travel 300,000,000 m/s s = 660 m. Due to time dilation, the moving muons last much longer and can reach the surface of the Earth before they decay. Length Contraction moving rods are measured to be shorter than when measured at rest. Think about the muons. Consider those created in the upper atmosphere at nearly the speed of light. In their own rest frame they don t last very long. In their rest frame, the surface of the Earth is rushing up to meet them at nearly the speed of light. Since they only last for 2.2 microseconds in their rest frame, how does the surface of the Earth reach them before they decay? In their frame, the distance between them and the surface of the Earth is shortened Length Contraction: So far we have been discussing kinematics how coordinates and times change. 2. Time Dilation Moving clocks run slow. where t is the time between ticks in the moving clock, t 0 is the time between ticks for the clock at rest, v is the speed of the clock, and c = speed of light. Has been tested: 1. Atomic clocks, synchronized, and then one sent on a plane trip for 24 hours, brought back disagree just as shown above. 2. GPS takes this into account. 3. Muons are unstable particles with a lifetime of 2.2 s. They last longer when their lifetimes are measured while they are in motion. The time dilation relation predicts, within experimental error, what is observed for the lifetime of the moving muons.

11 Length Contraction Muons are created in the upper atmosphere due to collisions between cosmic rays and molecules of air. These muons get to the surface of the Earth and form about 75% of the background radiation at the surface. But traveling a the speed of light for 2.2 s, they would only be able to travel a few hundred meters and wouldn t make it to the surface of the Earth. They get here due to time dilation the rapidly moving muons last long enough to make to the surface. Consider the rest frame of the muons in this frame, they last for only their 2.2- s lifetimes with the Earth rushing up to meet them at near the speed of light. The Earth is only going to move a few hundred meters in the 2.2 s how does it reach the muons before they decay? The distance from the Earth to the muons, in the muon rest frame, has shrunk or contracted to a few hundred meters. Moving rods are shorter. where L 0 is the rest length of the rod and L, the moving length. General Theory of Relativity GR Two Postulates of the General Theory of Relativity: 1. The laws of physics are the same in all frames of reference. 2. The principle of equivalence. Three statements of the principle of equivalence: 1. The inertial mass (the one that appears in Newton s second law, F = ma) is the same as the gravitational mass (the one that appears in Newton s law of gravity). 2. No experiment can be done in a closed elevator that will distinguish between being in free fall in a gravitational field or moving with constant velocity in gravity-free space. 3. No experiment can be done in a closed elevator that will distinguish between being at rest in a gravitational field or having a uniform acceleration in gravity-free space.

For instance, due to the solar wind, the Sun will lose about 0.1% of its mass over its main sequence existence.

For instance, due to the solar wind, the Sun will lose about 0.1% of its mass over its main sequence existence. 7/7 For instance, due to the solar wind, the Sun will lose about 0.1% of its mass over its main sequence existence. Once a star evolves off the main sequence, its mass changes more drastically. Some stars

More information

7/9. What happens to a star depends almost completely on the mass of the star. Mass Categories: Low-Mass Stars 0.2 solar masses and less

7/9. What happens to a star depends almost completely on the mass of the star. Mass Categories: Low-Mass Stars 0.2 solar masses and less 7/9 What happens to a star depends almost completely on the mass of the star. Mass Categories: Low-Mass Stars 0.2 solar masses and less Medium-Mass Stars 0.2 solar masses up to between 2 and 3 solar masses.

More information

Stellar Astronomy Sample Questions for Exam 4

Stellar Astronomy Sample Questions for Exam 4 Stellar Astronomy Sample Questions for Exam 4 Chapter 15 1. Emission nebulas emit light because a) they absorb high energy radiation (mostly UV) from nearby bright hot stars and re-emit it in visible wavelengths.

More information

Supernovae, Neutron Stars, Pulsars, and Black Holes

Supernovae, Neutron Stars, Pulsars, and Black Holes Supernovae, Neutron Stars, Pulsars, and Black Holes Massive stars and Type II supernovae Massive stars (greater than 8 solar masses) can create core temperatures high enough to burn carbon and heavier

More information

Ch. 16 & 17: Stellar Evolution and Death

Ch. 16 & 17: Stellar Evolution and Death Ch. 16 & 17: Stellar Evolution and Death Stars have lives: born, evolve, die Mass determines stellar evolution: Really Low Mass (0.08 to 0.4 M sun ) Low Mass: (0.4 to 4 M sun ) Long lives High Mass (4

More information

Astronomy 104: Second Exam

Astronomy 104: Second Exam Astronomy 104: Second Exam Stephen Lepp October 29, 2014 Each question is worth 2 points. Write your name on this exam and on the scantron. Short Answer A The Sun is powered by converting hydrogen to what?

More information

Astronomy Notes Chapter 13.notebook. April 11, 2014

Astronomy Notes Chapter 13.notebook. April 11, 2014 All stars begin life in a similar way the only difference is in the rate at which they move through the various stages (depends on the star's mass). A star's fate also depends on its mass: 1) Low Mass

More information

TA feedback forms are online!

TA feedback forms are online! 1 Announcements TA feedback forms are online! find the link at the class website. Please take 5 minutes to tell your TAs your opinion. In case you did not notice, the Final is set for 03/21 from 12:00-3:00

More information

The interpretation is that gravity bends spacetime and that light follows the curvature of space.

The interpretation is that gravity bends spacetime and that light follows the curvature of space. 7/8 General Theory of Relativity GR Two Postulates of the General Theory of Relativity: 1. The laws of physics are the same in all frames of reference. 2. The principle of equivalence. Three statements

More information

Dark Matter. About 90% of the mass in the universe is dark matter Initial proposals: MACHOs: massive compact halo objects

Dark Matter. About 90% of the mass in the universe is dark matter Initial proposals: MACHOs: massive compact halo objects 1 Dark Matter About 90% of the mass in the universe is dark matter Initial proposals: MACHOs: massive compact halo objects Things like small black holes, planets, other big objects They must be dark (so

More information

Death of stars is based on. one thing mass.

Death of stars is based on. one thing mass. Death of stars is based on one thing mass. Not the mass they have when born, but the mass they have when they die. Star Death for mass 1.4 solar masses and less. These stars started big 7.5-10 solar masses.

More information

Gravity simplest. fusion

Gravity simplest. fusion Gravity simplest fusion The life of a star has a complex relationship with gravity: 1. Gravity is what brings the original dust together to make a star 2. Gravity wants to crush the star Gravity pulls

More information

Comparing a Supergiant to the Sun

Comparing a Supergiant to the Sun The Lifetime of Stars Once a star has reached the main sequence stage of it life, it derives its energy from the fusion of hydrogen to helium Stars remain on the main sequence for a long time and most

More information

7/5. Consequences of the principle of equivalence (#3) 1. Gravity is a manifestation of the curvature of space.

7/5. Consequences of the principle of equivalence (#3) 1. Gravity is a manifestation of the curvature of space. 7/5 Consequences of the principle of equivalence (#3) 1. Gravity is a manifestation of the curvature of space. Follow the path of a light pulse in an elevator accelerating in gravityfree space. The dashed

More information

Stars and Galaxies 1

Stars and Galaxies 1 Stars and Galaxies 1 Characteristics of Stars 2 Star - body of gases that gives off great amounts of radiant energy as light and heat 3 Most stars look white but are actually different colors Antares -

More information

Directed Reading A. Section: The Life Cycle of Stars TYPES OF STARS THE LIFE CYCLE OF SUNLIKE STARS A TOOL FOR STUDYING STARS.

Directed Reading A. Section: The Life Cycle of Stars TYPES OF STARS THE LIFE CYCLE OF SUNLIKE STARS A TOOL FOR STUDYING STARS. Skills Worksheet Directed Reading A Section: The Life Cycle of Stars TYPES OF STARS (pp. 444 449) 1. Besides by mass, size, brightness, color, temperature, and composition, how are stars classified? a.

More information

Astro 1050 Fri. Apr. 10, 2015

Astro 1050 Fri. Apr. 10, 2015 Astro 1050 Fri. Apr. 10, 2015 Today: Continue Ch. 13: Star Stuff Reading in Bennett: For Monday: Finish Chapter 13 Star Stuff Reminders: Ch. 12 HW now on Mastering Astronomy, due Monday. Ch. 13 will be

More information

The Bizarre Stellar Graveyard

The Bizarre Stellar Graveyard The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White dwarfs

More information

Dead & Variable Stars

Dead & Variable Stars Dead & Variable Stars Supernovae Death of massive Stars As the core collapses, it overshoots and bounces A shock wave travels through the star and blows off the outer layers, including the heavy elements

More information

Chapters 12 and 13 Review: The Life Cycle and Death of Stars. How are stars born, and how do they die? 4/1/2009 Habbal Astro Lecture 27 1

Chapters 12 and 13 Review: The Life Cycle and Death of Stars. How are stars born, and how do they die? 4/1/2009 Habbal Astro Lecture 27 1 Chapters 12 and 13 Review: The Life Cycle and Death of Stars How are stars born, and how do they die? 4/1/2009 Habbal Astro 110-01 Lecture 27 1 Stars are born in molecular clouds Clouds are very cold:

More information

Missing words: mass hydrogen burning electrostatic repulsion. gravitationally hydrogen temperature protostar

Missing words: mass hydrogen burning electrostatic repulsion. gravitationally hydrogen temperature protostar Instructions Fill in the blanks of each frame using the list of missing words given. Cut out each frame and arrange them on your page in order, then stick them down. The first two frames are already in

More information

Life and Death of a Star. Chapters 20 and 21

Life and Death of a Star. Chapters 20 and 21 Life and Death of a Star Chapters 20 and 21 90 % of a stars life Most stars spend most of their lives on the main sequence. A star like the Sun, for example, after spending a few tens of millions of years

More information

Chapter 13 Notes The Deaths of Stars Astronomy Name: Date:

Chapter 13 Notes The Deaths of Stars Astronomy Name: Date: Chapter 13 Notes The Deaths of Stars Astronomy Name: Date: I. The End of a Star s Life When all the fuel in a star is used up, will win over pressure and the star will die nuclear fuel; gravity High-mass

More information

Stars with Mⵙ go through two Red Giant Stages

Stars with Mⵙ go through two Red Giant Stages Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Death of Stars Nuclear reactions in small stars How stars disperse carbon How low mass stars die The nature of white dwarfs

More information

Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9

Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9 Phys 0 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9 MULTIPLE CHOICE 1. We know that giant stars are larger in diameter than the sun because * a. they are more luminous but have about the

More information

Lecture 23 Stellar Evolution & Death (High Mass) November 21, 2018

Lecture 23 Stellar Evolution & Death (High Mass) November 21, 2018 Lecture 23 Stellar Evolution & Death (High Mass) November 21, 2018 1 2 High Mass Stars (M > 5 M ) Section 13.3 Bennett, The Essential Cosmic Perspective, 7 th ed. High mass stars have: More mass Greater

More information

The Night Sky. The Universe. The Celestial Sphere. Stars. Chapter 14

The Night Sky. The Universe. The Celestial Sphere. Stars. Chapter 14 The Night Sky The Universe Chapter 14 Homework: All the multiple choice questions in Applying the Concepts and Group A questions in Parallel Exercises. Celestial observation dates to ancient civilizations

More information

Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti

Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti INSTRUCTIONS: Please, use the `bubble sheet and a pencil # 2 to answer the exam questions, by marking

More information

Chapter 18 The Bizarre Stellar Graveyard

Chapter 18 The Bizarre Stellar Graveyard Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White

More information

High Mass Stars. Dr Ken Rice. Discovering Astronomy G

High Mass Stars. Dr Ken Rice. Discovering Astronomy G High Mass Stars Dr Ken Rice High mass star formation High mass star formation is controversial! May form in the same way as low-mass stars Gravitational collapse in molecular clouds. May form via competitive

More information

Chapter 14: The Bizarre Stellar Graveyard. Copyright 2010 Pearson Education, Inc.

Chapter 14: The Bizarre Stellar Graveyard. Copyright 2010 Pearson Education, Inc. Chapter 14: The Bizarre Stellar Graveyard Assignments 2 nd Mid-term to be held Friday Nov. 3 same basic format as MT1 40 mult. choice= 80 pts. 4 short answer = 20 pts. Sample problems on web page Origin

More information

Chapter 18 The Bizarre Stellar Graveyard. White Dwarfs. What is a white dwarf? Size of a White Dwarf White Dwarfs

Chapter 18 The Bizarre Stellar Graveyard. White Dwarfs. What is a white dwarf? Size of a White Dwarf White Dwarfs Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White

More information

The Stellar Graveyard Neutron Stars & White Dwarfs

The Stellar Graveyard Neutron Stars & White Dwarfs The Stellar Graveyard Neutron Stars & White Dwarfs White Dwarfs White dwarfs are the remaining cores of low-mass (M < 8M sun ) stars Electron degeneracy pressure supports them against gravity Density ~

More information

Introductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM

Introductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M

More information

Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008

Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Wed, July 16 MW galaxy, then review. Start with ECP3Ch14 2 through 8 Then Ch23 # 8 & Ch 19 # 27 & 28 Allowed Harlow Shapely to locate

More information

Neutron Stars, Black Holes, Pulsars and More

Neutron Stars, Black Holes, Pulsars and More Neutron Stars, Black Holes, Pulsars and More October 30, 2002 1) Star Clusters 2) Type II Supernova 3) Neutron Stars 4) Black Holes 5) More Gravity Announcements Extra Credit there is an extra credit assignment

More information

Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4

Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4 Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4 Key Ideas HR Diagrams of Star Clusters Ages from the Main Sequence Turn-off Open Clusters Young clusters of ~1000 stars Blue Main-Sequence

More information

NSCI 314 LIFE IN THE COSMOS

NSCI 314 LIFE IN THE COSMOS NSCI 314 LIFE IN THE COSMOS 2 BASIC ASTRONOMY, AND STARS AND THEIR EVOLUTION Dr. Karen Kolehmainen Department of Physics CSUSB COURSE WEBPAGE: http://physics.csusb.edu/~karen MOTIONS IN THE SOLAR SYSTEM

More information

Life and Evolution of a Massive Star. M ~ 25 M Sun

Life and Evolution of a Massive Star. M ~ 25 M Sun Life and Evolution of a Massive Star M ~ 25 M Sun Birth in a Giant Molecular Cloud Main Sequence Post-Main Sequence Death The Main Sequence Stars burn H in their cores via the CNO cycle About 90% of a

More information

Life and Death of a Star 2015

Life and Death of a Star 2015 Life and Death of a Star 2015 Name Date 1. In the main-sequence, the core is slowly shrinking because A. the mass of the star is slowly increasing B. hydrogen fusing to helium makes the core more dense

More information

Review: HR Diagram. Label A, B, C respectively

Review: HR Diagram. Label A, B, C respectively Stellar Evolution Review: HR Diagram Label A, B, C respectively A C B a) A: White dwarfs, B: Giants, C: Main sequence b) A: Main sequence, B: Giants, C: White dwarfs c) A: Main sequence, B: White Dwarfs,

More information

Heading for death. q q

Heading for death. q q Hubble Photos Credit: NASA, The Hubble Heritage Team (STScI/AURA) Heading for death. q q q q q q Leaving the main sequence End of the Sunlike star The helium core The Red-Giant Branch Helium Fusion Helium

More information

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Choose the answer that best completes the question. Read each problem carefully and read through all the answers.

More information

High Mass Stars and then Stellar Graveyard 7/16/09. Astronomy 101

High Mass Stars and then Stellar Graveyard 7/16/09. Astronomy 101 High Mass Stars and then Stellar Graveyard 7/16/09 Astronomy 101 Astronomy Picture of the Day Astronomy 101 Something Cool Betelgeuse Astronomy 101 Outline for Today Astronomy Picture of the Day Something

More information

X Rays must be viewed from space used for detecting exotic objects such as neutron stars and black holes also observing the Sun.

X Rays must be viewed from space used for detecting exotic objects such as neutron stars and black holes also observing the Sun. 6/25 How do we get information from the telescope? 1. Galileo drew pictures. 2. With the invention of photography, we began taking pictures of the view in the telescope. With telescopes that would rotate

More information

First: Some Physics. Tides on the Earth. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath. 1.

First: Some Physics. Tides on the Earth. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath. 1. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath First: Some Physics 1. Tides 2. Degeneracy Pressure Concept 1: How does gravity cause tides? R F tides

More information

Stars and their properties: (Chapters 11 and 12)

Stars and their properties: (Chapters 11 and 12) Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using

More information

Chapter 18 Lecture. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.

Chapter 18 Lecture. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc. Chapter 18 Lecture The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to

More information

Chapter 14: The Bizarre Stellar Graveyard

Chapter 14: The Bizarre Stellar Graveyard Lecture Outline Chapter 14: The Bizarre Stellar Graveyard 14.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf?

More information

10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure

10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure 10/26/16 Lecture Outline 13.1 Star Birth Chapter 13: Star Stuff How do stars form? Our goals for learning: How do stars form? How massive are newborn stars? Star-Forming Clouds Stars form in dark clouds

More information

Protostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium

Protostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium Protostars on the HR Diagram Once a protostar is hot enough to start, it can blow away the surrounding gas Then it is visible: crosses the on the HR diagram The more the cloud, the it will form stars Lifetimes

More information

White dwarfs are the remaining cores of dead stars. Electron degeneracy pressure supports them against the crush of gravity. The White Dwarf Limit

White dwarfs are the remaining cores of dead stars. Electron degeneracy pressure supports them against the crush of gravity. The White Dwarf Limit The Bizarre Stellar Graveyard Chapter 18 Lecture The Cosmic Perspective 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? Seventh

More information

Lecture 16: The life of a low-mass star. Astronomy 111 Monday October 23, 2017

Lecture 16: The life of a low-mass star. Astronomy 111 Monday October 23, 2017 Lecture 16: The life of a low-mass star Astronomy 111 Monday October 23, 2017 Reminders Online homework #8 due Monday at 3pm Exam #2: Monday, 6 November 2017 The Main Sequence ASTR111 Lecture 16 Main sequence

More information

8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars

8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars Classifying Stars In the early 1900s, Ejnar Hertzsprung and Henry Russell made some important observations. They noticed that, in general, stars with higher temperatures also have brighter absolute magnitudes.

More information

A100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy

A100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy A100 Exploring the Universe: Stellar Remnants Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu October 28, 2014 Read: S3, Chap 18 10/28/14 slide 1 Exam #2: November 04 One week from today!

More information

L = 4 d 2 B p. 4. Which of the letters at right corresponds roughly to where one would find a red giant star on the Hertzsprung-Russell diagram?

L = 4 d 2 B p. 4. Which of the letters at right corresponds roughly to where one would find a red giant star on the Hertzsprung-Russell diagram? Fall 2016 Astronomy - Test 3 Test form B Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form B on the answer sheet. Write your name above as well.

More information

L = 4 d 2 B p. 1. Which outer layer of the Sun has the highest temperature? A) Photosphere B) Corona C) Chromosphere D) Exosphere E) Thermosphere

L = 4 d 2 B p. 1. Which outer layer of the Sun has the highest temperature? A) Photosphere B) Corona C) Chromosphere D) Exosphere E) Thermosphere Fall 2016 Astronomy - Test 3 Test form A Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form A on the answer sheet. Write your name above as well.

More information

11/1/16. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard

11/1/16. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard Important Stuff (Section 001: 9:45 am) The Second Midterm is Thursday, November 10 The Second Midterm will be given in a different room: Willey 175 Bring 2 pencils and a photo-id. In accordance with the

More information

Announcement: Quiz Friday, Oct 31

Announcement: Quiz Friday, Oct 31 Announcement: Quiz Friday, Oct 31 What is the difference between the giant, horizontal, and asymptotic-giant branches? What is the Helium flash? Why can t high-mass stars support themselves in hydrostatic

More information

Late stages of stellar evolution for high-mass stars

Late stages of stellar evolution for high-mass stars Late stages of stellar evolution for high-mass stars Low-mass stars lead a relatively peaceful life in their old age: although some may gently blow off their outer envelopes to form beautiful planetary

More information

Chapter 12 Review. 2) About 90% of the star's total life is spent on the main sequence. 2)

Chapter 12 Review. 2) About 90% of the star's total life is spent on the main sequence. 2) Chapter 12 Review TRUE/FALSE. Write 'T' if the statement is true and 'F' if the statement is false. 1) As a main-sequence star, the Sun's hydrogen supply should last about 10 billion years from the zero-age

More information

Physics HW Set 3 Spring 2015

Physics HW Set 3 Spring 2015 1) If the Sun were replaced by a one solar mass black hole 1) A) life here would be unchanged. B) we would still orbit it in a period of one year. C) all terrestrial planets would fall in immediately.

More information

Announcements. L! m 3.5 BRIGHT FAINT. Mass Luminosity Relation: Why? Homework#3 will be handed out at the end of this lecture.

Announcements. L! m 3.5 BRIGHT FAINT. Mass Luminosity Relation: Why? Homework#3 will be handed out at the end of this lecture. Announcements BRIGHT Homework#3 will be handed out at the end of this lecture. Due October 14 (next Thursday) Review of Mid-term exam will be handed out Tuesday. Mid-term exam will be variants (if not

More information

Prentice Hall EARTH SCIENCE

Prentice Hall EARTH SCIENCE Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 25 Beyond Our Solar System 25.1 Properties of Stars Characteristics of Stars A constellation is an apparent group of stars originally named for mythical

More information

PHYS 1401: Descriptive Astronomy Notes: Chapter 12

PHYS 1401: Descriptive Astronomy Notes: Chapter 12 CHAPTER 12: STELLAR EVOLUTION 12.1: LEAVING THE MAIN SEQUENCE Stars and the Scientific Method You cannot observe a single star from birth to death You can observe a lot of stars in a very short period

More information

The life of a low-mass star. Astronomy 111

The life of a low-mass star. Astronomy 111 Lecture 16: The life of a low-mass star Astronomy 111 Main sequence membership For a star to be located on the Main Sequence in the H-R diagram: must fuse Hydrogen into Helium in its core. must be in a

More information

Beyond the Solar System 2006 Oct 17 Page 1 of 5

Beyond the Solar System 2006 Oct 17 Page 1 of 5 I. Stars have color, brightness, mass, temperature and size. II. Distances to stars are measured using stellar parallax a. The further away, the less offset b. Parallax angles are extremely small c. Measured

More information

AST 101 Introduction to Astronomy: Stars & Galaxies

AST 101 Introduction to Astronomy: Stars & Galaxies AST 101 Introduction to Astronomy: Stars & Galaxies Life and Death of High Mass Stars (M > 8 M sun ) REVIEW Last stage: Iron core surrounded by shells of increasingly lighter elements. REVIEW When mass

More information

It is possible for a couple of elliptical galaxies to collide and become a spiral and for two spiral galaxies to collide and form an elliptical.

It is possible for a couple of elliptical galaxies to collide and become a spiral and for two spiral galaxies to collide and form an elliptical. 7/16 Ellipticals: 1. Very little gas and dust an no star formation. 2. Composed of old stars. 3. Masses range from hundreds of thousands to 10's of trillions of solar masses. 4. Sizes range from 3000 ly

More information

ASTRONOMY 1 EXAM 3 a Name

ASTRONOMY 1 EXAM 3 a Name ASTRONOMY 1 EXAM 3 a Name Identify Terms - Matching (20 @ 1 point each = 20 pts.) Multiple Choice (25 @ 2 points each = 50 pts.) Essays (choose 3 of 4 @ 10 points each = 30 pt 1.Luminosity D 8.White dwarf

More information

Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused

More information

LIFE CYCLE OF A STAR

LIFE CYCLE OF A STAR LIFE CYCLE OF A STAR First stage = Protostar PROTOSTAR Cloud of gas and dust many light-years across Gravity tries to pull the materials together Eventually, at the center of the ball of dust and gas,

More information

20. Stellar Death. Interior of Old Low-Mass AGB Stars

20. Stellar Death. Interior of Old Low-Mass AGB Stars 20. Stellar Death Low-mass stars undergo three red-giant stages Dredge-ups bring material to the surface Low -mass stars die gently as planetary nebulae Low -mass stars end up as white dwarfs High-mass

More information

RELATIVITY. The End of Physics? A. Special Relativity. 3. Einstein. 2. Michelson-Morley Experiment 5

RELATIVITY. The End of Physics? A. Special Relativity. 3. Einstein. 2. Michelson-Morley Experiment 5 1 The End of Physics? RELATIVITY Updated 01Aug30 Dr. Bill Pezzaglia The following statement made by a Nobel prize winning physicist: The most important fundamental laws and facts of physical science have

More information

Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.

Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc. Chapter 17 Lecture The Cosmic Perspective Seventh Edition Star Stuff Star Stuff 17.1 Lives in the Balance Our goals for learning: How does a star's mass affect nuclear fusion? How does a star's mass affect

More information

ASTR Midterm 1 Phil Armitage, Bruce Ferguson

ASTR Midterm 1 Phil Armitage, Bruce Ferguson ASTR 1120-001 Midterm 1 Phil Armitage, Bruce Ferguson FIRST MID-TERM EXAM FEBRUARY 16 th 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.

More information

Protostars evolve into main-sequence stars

Protostars evolve into main-sequence stars Understanding how stars evolve requires both observation and ideas from physics The Lives of Stars Because stars shine by thermonuclear reactions, they have a finite life span That is, they fuse lighter

More information

Astronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. Name: Period: Date: Astronomy Ch. 22 Neutron Stars and Black Holes MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) In a neutron star, the core

More information

Introduction to Astronomy. Lecture 8: The Death of Stars White Dwarfs, Neutron Stars, and Black Holes

Introduction to Astronomy. Lecture 8: The Death of Stars White Dwarfs, Neutron Stars, and Black Holes Introduction to Astronomy Lecture 8: The Death of Stars White Dwarfs, Neutron Stars, and Black Holes Continued from Last Week Lecture 7 Observing Stars Clusters of stars Some clouds start breaking into

More information

the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes

the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes The spectral lines of stars tell us their approximate composition Remember last year in Physics?

More information

Astronomy 10 Test #2 Practice Version

Astronomy 10 Test #2 Practice Version Given (a.k.a. `First ) Name(s): Family (a.k.a. `Last ) name: ON YOUR PARSCORE: `Bubble your name, your student I.D. number, and your multiple-choice answers. I will keep the Parscore forms. ON THIS TEST

More information

The Life and Death of Stars

The Life and Death of Stars The Life and Death of Stars What is a Star? A star is a sphere of plasma gas that fuses atomic nuclei in its core and so emits light The name star can also be tagged onto a body that is somewhere on the

More information

Stellar Evolution: Outline

Stellar Evolution: Outline Stellar Evolution: Outline Interstellar Medium (dust) Hydrogen and Helium Small amounts of Carbon Dioxide (makes it easier to detect) Massive amounts of material between 100,000 and 10,000,000 solar masses

More information

ASTR 200 : Lecture 20. Neutron stars

ASTR 200 : Lecture 20. Neutron stars ASTR 200 : Lecture 20 Neutron stars 1 Equation of state: Degenerate matter We saw that electrons exert a `quantum mechanical' pressure. This is because they are 'fermions' and are not allowed to occupy

More information

Chapter 13 2/19/2014. Lecture Outline Neutron Stars. Neutron Stars and Black Holes Neutron Stars. Units of Chapter

Chapter 13 2/19/2014. Lecture Outline Neutron Stars. Neutron Stars and Black Holes Neutron Stars. Units of Chapter 13.1 Neutron Stars Lecture Outline Chapter 13 Neutron Stars and After a Type I supernova, little or nothing remains of the original star. After a Type II supernova, part of the core may survive. It is

More information

Outline. Stellar Explosions. Novae. Death of a High-Mass Star. Binding Energy per nucleon. Nova V838Mon with Hubble, May Dec 2002

Outline. Stellar Explosions. Novae. Death of a High-Mass Star. Binding Energy per nucleon. Nova V838Mon with Hubble, May Dec 2002 Outline Novae (detonations on the surface of a star) Supernovae (detonations of a star) The Mystery of Gamma Ray Bursts (GRBs) Sifting through afterglows for clues! Stellar Explosions Novae Nova V838Mon

More information

LIFE CYCLE OF A STAR

LIFE CYCLE OF A STAR LIFE CYCLE OF A STAR First stage = Protostar PROTOSTAR Cloud of gas and dust many light-years across Gravity tries to pull the materials together Eventually, at the center of the ball of dust and gas,

More information

Astronomy 1 Fall 2016

Astronomy 1 Fall 2016 Astronomy 1 Fall 2016 Lecture 14; November 10, 2016 Previously on Astro 1 Late evolution and death of intermediate-mass stars (about 0.4 M to about 4 M ): red giant when shell hydrogen fusion begins, a

More information

Astronomy. Stellar Evolution

Astronomy. Stellar Evolution Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Stellar Evolution Main Sequence star changes during nuclear fusion What happens when the fuel runs out Old stars and second

More information

Astronomy 1144 Exam 3 Review

Astronomy 1144 Exam 3 Review Stars and Stellar Classification Astronomy 1144 Exam 3 Review Prof. Pradhan 1. What is a star s energy source, or how do stars shine? Stars shine by fusing light elements into heavier ones. During fusion,

More information

Properties of Stars. Characteristics of Stars

Properties of Stars. Characteristics of Stars Properties of Stars Characteristics of Stars A constellation is an apparent group of stars originally named for mythical characters. The sky contains 88 constellations. Star Color and Temperature Color

More information

11/1/17. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard

11/1/17. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard 11/1/17 Important Stuff (Section 001: 9:45 am) The Second Midterm is Thursday, November 9 The Second Midterm will be given in a different room: Willey 175 Bring 2 pencils and a photo-id. In accordance

More information

Before proceeding to Chapter 20 More on Cluster H-R diagrams: The key to the chronology of our Galaxy Below are two important HR diagrams:

Before proceeding to Chapter 20 More on Cluster H-R diagrams: The key to the chronology of our Galaxy Below are two important HR diagrams: Before proceeding to Chapter 20 More on Cluster H-R diagrams: The key to the chronology of our Galaxy Below are two important HR diagrams: 1. The evolution of a number of stars all formed at the same time

More information

Outline - March 18, H-R Diagram Review. Protostar to Main Sequence Star. Midterm Exam #2 Tuesday, March 23

Outline - March 18, H-R Diagram Review. Protostar to Main Sequence Star. Midterm Exam #2 Tuesday, March 23 Midterm Exam #2 Tuesday, March 23 Outline - March 18, 2010 Closed book Will cover Lecture 8 (Special Relativity) through Lecture 14 (Star Formation) only If a topic is in the book, but was not covered

More information

Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.

Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D. Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Stellar Deaths/Endpoints 13-2 Low Mass Stars ³ Like the Sun (< 2 M ) ² Live about 10 billion years (sun is middle aged) ² Create elements through Carbon, Nitrogen,

More information

Star Formation and Evolution

Star Formation and Evolution Star Formation and Evolution Low and Medium Mass Stars Four Components of the Interstellar Medium Component Temperature Density (K) (atoms/cm 3 ) HI Clouds 50 150 1 1000 Intercloud Medium 10 3-10 4 0.01

More information

Low mass stars. Sequence Star Giant. Red. Planetary Nebula. White Dwarf. Interstellar Cloud. White Dwarf. Interstellar Cloud. Planetary Nebula.

Low mass stars. Sequence Star Giant. Red. Planetary Nebula. White Dwarf. Interstellar Cloud. White Dwarf. Interstellar Cloud. Planetary Nebula. Low mass stars Interstellar Cloud Main Sequence Star Red Giant Planetary Nebula White Dwarf Interstellar Cloud Main Sequence Star Red Giant Planetary Nebula White Dwarf Low mass stars Interstellar Cloud

More information

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. HW3 Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused by falling matter from the atmosphere of

More information

Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM

Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM RLM 15.216B (Backup RLM 15.202A) Reading: Chapter 6

More information

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. Lecture 4 Stars The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. X-ray ultraviolet infrared radio To understand

More information